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The structure of cometary dust is a tracer of growth processes in theformation of planetesimals. Instrumentation on board the Rosetta mission tocomet 67P/Churyumov- Gerasimenko captured dust particles and analysed them insitu. However, these deposits are a product of a collision within theinstrument. We conducted laboratory experiments with cometary dust analogues,simulating the collection process by Rosetta instruments (specifically COSIMA,MIDAS). In Paper I we reported that velocity is a key driver in determining theappearance of deposits. Here in Paper II we use materials with differentmonomer sizes, and study the effect of tensile strength on the appearance ofdeposits. We find that mass transfer efficiency increases from $\sim$1 up to$\sim$10% with increasing monomer diameter from 0.3 $\mu$m to 1.5 $\mu$m (i.e.tensile strength decreasing from $\sim$12 to $\sim$3 kPa), and velocitiesincreasing from 0.5 to 6 m/s. Also, the relative abundance of small fragmentsafter impact is higher for material with higher tensile strength. Thedegeneracy between the effects of velocity and material strength may be liftedby performing a closer study of the deposits. This experimental method makes itpossible to estimate the mass transfer efficiency in the COSIMA instrument.Extrapolating these results implies that more than half of the dust collectedduring the Rosetta mission has not been imaged. We analysed two COSIMA targetscontaining deposits from single collisions. The collision that occurred closestto perihelion passage led to more small fragments on the target.

The footprint of cometary dust analogues: II. Morphology as a tracer of tensile strength and application to dust collection by the Rosetta spacecraft